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B.R.N.O. Contributions #36, Times of minima
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| Spectroscopic and photometric observations of the selected Algol-type binaries - IV. V799Cassiopeiae, BX Piscium and HD 172189
We present new radial velocities and UBV photometric observations ofthree eclipsing binaries, V799Cas, BXPsc and HD172189, in order toincrease the number of close binaries with absolute parametersdetermined accurately. Standard wide-band indices for the systems andcomparison stars were determined accurately. Using the times ofmid-eclipses, new ephemerides are calculated for three systems. V799Casand HD172189 consist of two well-detached components in eccentricorbits. BXPsc is a single-lined eclipsing binary which consists of alate-A and an early-K star. The effective temperatures of the hottercomponents and reddening of the systems have been estimated from Johnsonwide-band UBV photometric calibrations. The UBV photometric data andradial velocities were analysed simultaneously for the systems'parameters using Wilson-Devinney code. The masses have been found to be3.08 +/- 0.40, 2.97 +/- 0.40; 1.85 +/- 0.14, 0.80 +/- 0.08; 2.06 +/-0.15, 1.87 +/- 0.14 Msolar for the primary and secondarystars of V799Cas, BXPsc and HD172189, respectively. The radii of thecomponents are derived in the case of V799Cas: 3.23 +/- 0.14, 3.20 +/-0.14; in those of BXPsc: 3.76 +/- 0.14, 2.18 +/- 0.09; and HD172189:4.01 +/- 0.09, 2.97 +/- 0.07 Rsolar. We have calculated thedistances to the systems of V799Cas, BXPsc and HD172189 as 607 +/- 35,213 +/- 6 and 432 +/- 12 pc, respectively, using bolometric magnitudesand empirical bolometric corrections for the component stars. The modelpredictions match the measured properties of V779Cas, BXPsc and HD172189for an age of 250 Myr, 1 Gyr and 890 Myr, respectively. A subsolarfractional metal abundance, Z ~ 0.008, provides a better match to theabsolute parameters of all three systems.Based on observations collected at the Catania Astrophysical Observatory(Italy), Ege University Observatory (?zmir, Turkey) and DavidDunlap Observatory (Canada).E-mail: cibanoglu@ege.edu.tr
| B.R.N.O. Contributions #34
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| A new catalogue of eclipsing binary stars with eccentric orbits
A new catalogue of eclipsing binary stars with eccentric orbits ispresented. The catalogue lists the physical parameters (includingapsidal motion parameters) of 124 eclipsing binaries with eccentricorbits. In addition, the catalogue also contains a list of 150 candidatesystems, about which not much is known at present.Full version of the catalogue is available online (see the SupplementaryMaterial section at the end of this paper) and in electronic form at theCDS via http://cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/MNRAS/(vol)/ (page)E-mail: ibulut@comu.edu.tr
| CCD Times of Minima of Selected Eclipsing Binaries
374 CCD minima observations of 187 eclipsing binaries are presented. Theobserved stars were chosen mainly from catalogue BRKA of observingprogramme of Variable Star Section of CAS.
| A catalogue of eclipsing variables
A new catalogue of 6330 eclipsing variable stars is presented. Thecatalogue was developed from the General Catalogue of Variable Stars(GCVS) and its textual remarks by including recently publishedinformation about classification of 843 systems and making correspondingcorrections of GCVS data. The catalogue1 represents thelargest list of eclipsing binaries classified from observations.
| Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
| The 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| The local system of early type stars - Spatial extent and kinematics
Published uvby and H-beta photometric data and proper motions arecompiled and analyzed to characterize the structure and kinematics ofthe bright early-type O-A0 stars in the solar vicinity, with a focus onthe Gould belt. The selection and calibration techniques are explained,and the data are presented in extensive tables and graphs and discussedin detail. The Gould belt stars of age less than 20 Myr are shown togive belt inclination 19 deg to the Galactic plane and node-lineorientation in the direction of Galactic rotation, while the symmetricaldistribution about the Galactic plane and kinematic properties (purecircular differential rotation) of the belt stars over 60 Myr oldresemble those of fainter nonbelt stars of all ages. The unresolveddiscrepancy between the expansion observed in the youngest nearby starsand the predictions of simple models of expansion from a point isattributed to the inhomogeneous distribution of interstellar matter.
| Four-color and H-beta photometry for O-A0 type stars in three regions near the galactic equator
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1982A&AS...49..561W&db_key=AST
| A spectrophotometric survey of stars along the Milky Way. IV
In the present paper a catalogue of spectrophotometric quantities,spectral types, monochromatic magnitudes and colour equivalents is givenfor all stars brighter than the magnitude m4400 = 10.5 in aregion of the Milky Way in Perseus. No absorption is found for starscloser than about r = 100 pc. The absorbing clouds are situated atdistances closer than 1 kpc and at about 2.5 kpc in the local arm andthe Perseus arm, respectively. The space between the two arms is freefrom absorption. It is also concluded that the Perseus arm continuesbeyond l = 140 deg, containing not only hydrogen gas but also dust to atleast l = 150 deg), while the content of OB stars decreases abruptly atl = 140 deg.
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Observation and Astrometry data
| Constellation: | Cassiopeia |
| Right ascension: | 03h05m27.55s |
| Declination: | +61°39'17.7" |
| Apparent magnitude: | 8.82 |
| Distance: | 322.581 parsecs |
| Proper motion RA: | -4.5 |
| Proper motion Dec: | -1.8 |
| B-T magnitude: | 8.999 |
| V-T magnitude: | 8.835 |
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